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We use the SIMBA suite of cosmological hydrodynamical simulations toinvestigate the importance of various stellar and AGN feedback mechanisms inpartitioning the cosmic baryons between the intergalactic (IGM) andcircumgalactic (CGM) media in the $z\leq 1$ Universe. We identify the AGN jetsas the most prominent mechanism for the redistribution of baryons between theCGM and large-scale IGM. In contrast to the full feedback models, deactivatingAGN jets results in $\approx15-20$ per cent drop in fraction of baryons thatreside in the IGM and a consequent increase of baryon fraction in the CGM by$\approx 50$ per cent. Additionally, we find that stellar feedback mechanismsmodify the baryon partition between IGM and CGM on a $10$ per cent level. Wefurther examine the physical properties of simulated haloes in different massbins, and their response to various feedback models. On average, a sixfolddecrease in the CGM mass fraction due to the inclusion of feedback fromAGN-driven jets is detected in $10^{12}M_{\odot} \leq M_{\rm 200} \leq10^{14}M_{\odot}$ haloes. Examination of the average radial gas densityprofiles of $M_{200} > 10^{12}M_{\odot}$ haloes reveals up to an order ofmagnitude decrease in gas densities due to the AGN jet feedback. We compare gasdensity profiles from SIMBA simulations to the predictions of the analyticalmodified NFW model, and show that the latter provides a reasonableapproximation of the gas radial profiles within the virial radii of the fullrange of halo masses when rescaled by the CGM fraction of the halo. Therelative partitioning of cosmic baryons and, subsequently, the feedback modelscan be constrained observationally with fast radio bursts (FRBs) in upcomingsurveys.

The Cosmic Baryon Partition between the IGM and CGM in the SIMBA Simulations